H2 in interstellar and extragalactic ices: infrared characteristics, ultraviolet production, and implications.
H2 in interstellar and extragalactic ices: infrared characteristics, ultraviolet production, and implications.
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星际和河外冰中的 H2：红外特征、紫外产生和影响。
DOI：
10.1086/186861
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发表时间：
1993
期刊：
影响因子：
--
通讯作者：
L. Allamandola
中科院分区：
文献类型：
--
作者：
S. Sandford;L. Allamandola
H2是宇宙中最丰富的分子。我们证明，这种分子可能是星际和可能的星系际冰的重要组成部分，既因为它可以在原位形成，在冰内，因为气相H2可以冻结到尘埃颗粒在一些天体物理环境。介绍了含氢冰的冷凝-升华和红外光谱性质。我们表明，固体H2在H20丰富的冰可以检测到的红外吸收带在4137 cm-1（2.417微米）。测得H2与H2O冰的表面结合能为Δ Hs/k = 555 +/- 35 K。表面结合能可用于计算作为温度的函数的H2在晶粒表面上的停留时间。这些结果的一些影响被认为是。
H2 is the most abundant molecule in the universe. We demonstrate that this molecule may be an important component of interstellar and possibly intergalactic ices, both because it can be formed in situ, within the ices, and because gas phase H2 can freeze out onto dust grains in some astrophysical environments. The condensation-sublimation and infrared spectral properties of ices containing H2 are presented. We show that solid H2 in H20-rich ices can be detected by an infrared absorption band at 4137 cm-1 (2.417 micrometers). The surface binding energy of H2 to H2O ice was measured to the delta Hs/k = 555 +/- 35 K. Surface binding energies can be used to calculate the residence times of H2 on grain surfaces as a function of temperature. Some of the implications of these results are considered.